This investigation is devoted to the effects of nonadiabatic
resonant dynamic tides generated in a uniformly rotating stellar
component of a close binary. The companion is considered to move in a
fixed Keplerian orbit, and the effects of the centrifugal force and the
Coriolis force are neglected. Semi-analytical solutions for the
linear, nonadiabatic resonant dynamic tides are derived by means of a
two-time variable expansion procedure. The solution at the lowest
order of approximation consists of the resonantly excited oscillation
mode and displays a phase shift with respect to the tide-generating
potential. Expressions are established for the secular variations of
the semi-major axis, the orbital eccentricity, and the star's angular
velocity of rotation caused by the phase shift. The orders of
magnitude of these secular variations are considerably larger than
those derived earlier by Zahn (1977) for the limiting case of
dynamic tides with small frequencies. For a ZAMS star, an
orbital eccentricity , and orbital periods in the range from
2 to 5 days, numerous resonances of dynamic tides with second-degree
lower-order g+-modes are seen to induce secular variations of the
semi-major axis, the orbital eccentricity, and the star's angular
velocity of rotation with time scales shorter than the star's nuclear
life time.

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